Correlations between mass, stellar kinematics, and gas metallicity in EAGLE galaxies
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Correlations between mass, stellar kinematics, and gas metallicity in EAGLE galaxies. / Zenocratti, L. J.; De Rossi, M. E.; Lara-Lopez, M. A.; Theuns, T.
In: Monthly Notices of the Royal Astronomical Society, Vol. 496, No. 1, 07.2020, p. L33-L37.Research output: Contribution to journal › Letter › Research › peer-review
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TY - JOUR
T1 - Correlations between mass, stellar kinematics, and gas metallicity in EAGLE galaxies
AU - Zenocratti, L. J.
AU - De Rossi, M. E.
AU - Lara-Lopez, M. A.
AU - Theuns, T.
PY - 2020/7
Y1 - 2020/7
N2 - The metallicity of star-forming gas in galaxies from the EAGLE (Evolution and Assembly of GaLaxies and their Environments) simulations increases with stellar mass. Here, we investigate whether the scatter around this relation correlates with morphology and/or stellar kinematics. At redshift z = 0, galaxies with more rotational support have lower metallicities on average when the stellar mass is below M-* approximate to 10(10) M-circle dot. This trend inverts at higher values of M-*, when prolate galaxies show typically lower metallicity. At increasing redshifts, the trend between rotational support and metallicity becomes weaker at low stellar mass but more pronounced at high stellar mass. We argue that the secondary dependence of metallicity on stellar kinematics is another manifestation of the observed anticorrelation between metallicity and star formation rate at a given stellar mass. At low masses, such trends seem to be driven by the different star formation histories of galaxies and stellar feedback. At high masses, feedback from active galactic nuclei and galaxy mergers plays a dominant role.
AB - The metallicity of star-forming gas in galaxies from the EAGLE (Evolution and Assembly of GaLaxies and their Environments) simulations increases with stellar mass. Here, we investigate whether the scatter around this relation correlates with morphology and/or stellar kinematics. At redshift z = 0, galaxies with more rotational support have lower metallicities on average when the stellar mass is below M-* approximate to 10(10) M-circle dot. This trend inverts at higher values of M-*, when prolate galaxies show typically lower metallicity. At increasing redshifts, the trend between rotational support and metallicity becomes weaker at low stellar mass but more pronounced at high stellar mass. We argue that the secondary dependence of metallicity on stellar kinematics is another manifestation of the observed anticorrelation between metallicity and star formation rate at a given stellar mass. At low masses, such trends seem to be driven by the different star formation histories of galaxies and stellar feedback. At high masses, feedback from active galactic nuclei and galaxy mergers plays a dominant role.
KW - galaxies: abundances
KW - galaxies: evolution
KW - galaxies: high-redshift
KW - galaxies: star formation
KW - cosmology: theory
KW - STAR-FORMATION RATE
KW - FUNDAMENTAL RELATION
KW - SCALING RELATIONS
KW - EVOLUTION
KW - DEPENDENCE
KW - MORPHOLOGY
KW - ORIGIN
KW - SIMULATIONS
KW - PROJECT
KW - HALO
U2 - 10.1093/mnrasl/slaa085
DO - 10.1093/mnrasl/slaa085
M3 - Letter
VL - 496
SP - L33-L37
JO - Royal Astronomical Society. Monthly Notices
JF - Royal Astronomical Society. Monthly Notices
SN - 0035-8711
IS - 1
ER -
ID: 247983047